American Astronomical Society, Astrophysical Journal, (338), p. 424, 1989
DOI: 10.1086/167210
Cool Stars, Stellar Systems, and the Sun, p. 205-216
DOI: 10.1007/3-540-18653-0_134
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A new rotating stellar evolution code is developed and applied to the sun. A hydrostatic fully convective premain-sequence model is evolved to the age of the sun. As the model evolves, it accounts for angular-momentum loss via a magnetic wind and angular-momentum redistribution by rotationally induced instabilities. The resulting models have an oblateness in agreement with observed upper limits. The rotation curves show two main features: the outer layers exhibit minimal radial differential rotation, and a rapidly rotating central core is preserved. These basic features persist through a wide range of model parameters.